Nonetheless, hints that the relativistic radio lobes of the central AGN do have an impact on the metallicity distribution in groups have been obtained in a few objects. Perhaps the clearest example so far is that of AWM 4, where [1]} found a metal enhancement along the inner jet of the central dominant galaxy, NGC6051, corresponding to an excess mass of iron in the entrained gas of \(\sim 1.4\times 10^6\:\rm {M}_\odot \) . Another case is that of NGC4636, where [2]} report a plume of cool, metal-rich gas extending beyond a known AGN lobe to the southwest of the galaxy center, and interpret this to be the product of metal entrainment by past AGN activity. Less clear is the scenario in NGC4325; here [3]} reported an elongated Fe-rich filament to the south/southeast of the central galaxy which could be due to metal entrainment by the AGN; however, no X-ray cavity is found in this system that would confirm this interpretation. Finally, there are the interesting examples of rather clearly detected anticorrelations, i.e. a low metallicity corresponding to the radio lobes in NGC5813 [4]} and inner radio lobes of M49 [5]} – although, in both cases, only a single-temperature fit was used to create the 2D maps, hence the Fe bias may be the reason for these results.
